Issue |
A&A
Volume 686, June 2024
|
|
---|---|---|
Article Number | A121 | |
Number of page(s) | 9 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/202348895 | |
Published online | 04 June 2024 |
Simultaneous NICER and NuSTAR observations of the ultraluminous source NGC 4190 ULX-1
1
Instituto Argentino de Radioastronomía (CCT La Plata, CONICET; CICPBA; UNLP), C.C.5, (1894), Villa Elisa, Argentina
e-mail: jorgearielcombi@gmail.com
2
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, B1900FWA La Plata, Argentina
3
Instituto de Astrofísica de Canarias (IAC), Vía Láctea s/n, La Laguna, 38205 S/C de Tenerife, Spain
4
Departamento de Astrofísica, Universidad de La Laguna, La Laguna, 38205 S/C de Tenerife, Spain
5
Departamento de Física (EPS), Universidad de Jaén, Campus Las Lagunillas s/n, A3, 23071 Jaén, Spain
Received:
9
December
2023
Accepted:
18
March
2024
Aims. We present an X-ray analysis of three different XMM-Newton observations together with simultaneous NICER and NuSTAR observations of the ultraluminous X-ray source NGC 4190 ULX-1. Our goal is to constrain the structure of the accretion disk and the geometrical properties of the source.
Methods. We performed temporal and spectral analyses in the 0.4−30 keV energy range in which the source is significantly detected in dedicated XMM-Newton, NICER, and NuSTAR observations.
Results. The temporal analysis shows no flaring activity in the light curves. No pulsation is detected throughout. The source exhibits a typical ULX spectrum, which can be fitted with two thermal blackbody components plus a Comptonization tail at high energies. The luminosity–temperature (L − T) relation of each thermal spectral component is consistent with the L ∝ T2 relation expected from an advection-dominated supercritical disk.
Conclusions. We interpret these results as a super-Eddington accreting black hole seen almost face-on. A dense wind ejected from the disk obscures the central source, and a hot electron plasma is evacuated through the funnel formed above the hole. Geometric beaming is responsible for the ULX soft emission, whereas the hard tail is the result of the Comptonization of soft photons by the electrons ejected through the funnel.
Key words: accretion / accretion disks / stars: black holes / stars: individual: NGC 4190 ULX-1
© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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